A new classification of ex situ and in situ Galactic globular clusters based on a method trained on Milky Way analogues in the TNG50 cosmological simulations

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Volume 704 (December 2025)

A&A, 704 (2025) A81

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Table A.1

Impact of free parameters in our modelling

	Ex situ in 0.95 boundary %	In situ in 0.05 boundary %	N_exsitu	N_{mixing zone}	N_insitu
Fiducial model	81.21	76.4	67	38	55
Fixed disk potential	81.28	74.97	67	40	53
In situ tagged at z = 3	83.13	23.45	78	68	14
$M_{G C}^{ini} = 5 \times 10^{5}$ $\[M_{\mathrm{GC}}^{\text {ini}}=5 \times 10^{5}\]$ M_⊙	80.27	41	65	30	65
$M_{GC}^{ini} = 5 \times 10^{6}$ $\[M_{\text {GC}}^{\text {ini}}=5 \times 10^{6}\]$ M_⊙	81.38	96.5	68	49	43
Mass loss
(γ = 0.7 & t_0,⊙ = 10.7 Myr)	80.83	54.17	66	32	62

Notes: From left to right, the columns report, for each configuration: the percentage of simulated GCs classified as ex situ and in situ using the 0.95 and 0.05 decision boundaries, respectively, as well as the number of GCs identified as ex situ, in the mixing zone, and in situ. Our fiducial model assumes 10⁶ M_⊙ GCs tagged at z = 2 for in situ clusters and at z = 3 for ex situ ones, evolved in MW-like potentials without a disk component, with mass loss parametrized by γ = 0.62 and t_0,⊙ = 21.3 Myr. The fixed disk is modelled using a Miyamoto & Nagai (1975) potential with a mass of 6.8 × 10¹⁰ M_⊙, a scale length a = 3 kpc, and a scale height b = 280 pc, consistent with the MWPotential2014 used in Bovy (2015).

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